The similarities between chemical enrichment of the IGrM in lower-temperature groups and the ICM in massive objects is further supported by the shallow dependence of gas global metallicity on the system mass (or temperature).
In contrast to observational findings, where lower iron abundances were typically observed in group-size systems compared to clusters, [1]} report
a shallow, mildly anti-correlating, metallicity-temperature relation, employing semi-analytic models of galaxy evolution.
Simulation results, like those presented in [2]} and [3]}, also predict a shallow anti-relation between metallicity and temperature, that extends without breaks from clusters down to groups.
More recently, [4]}
compare the relation between temperature and iron abundance in the core (i.e. \(<0.1\,R_{500}\) ) of simulated groups and clusters with recent results from the CHEERS sample [5]},
also finding a shallow anti-correlation overall, with a mass-invariance of the IGrM and ICM iron abundance in cool-core clusters, as shown in Fig. REF .
In the Figure, in particular, the simulated data (star symbols) are reported together with the best-fit relation for the whole sample, and for the CC and NCC subsamples, with the former in better agreement with the CHEERS results .
[2]} show that a flat relation with temperature applies as well when abundance ratios relative to iron are investigated (e.g. O/Fe, Si/Fe, S/Fe etc.).
Interestingly, this is also in line with recent observational findings .
